Detection of Ultra-high energy neutrinos The First Light of the high energy neutrino astronomy
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1 Detection of Ultra-high energy neutrinos The First Light of the high energy neutrino astronomy Shigeru Yoshida Department of Physics Chiba University
2 the 1 st discovery of the PeV ν Bert Physical Review Letters 111, (2013) 1.04 PeV Ernie 1.14 PeV σ 2.8 excess on the atmospheric background very the 1 st indication of astrophysical ν
3 Cover-boy of Physical Review Letters
4 Cover-boy of Physical Review Letters
5 A proof of the PRL s high standard for publication The version submitted The version accepted
6 The challenge No clear correlations.. Two possibilities 1. Our hypotheses on the high energy cosmic ray emitters are totally wrong We may not be so smart. Arrival directions of UHE cosmic-rays measured by Auger and the Integral X-ray map (above) or the nearby clusters (arxiv D.Fargion et al) 2. Cannot handle pointing them back to their radiation points Magnetic field? Particle charge? Proton or even iron?
7 Solutions 1. Correct more and more events A super high statistics may resolve B, charge, and source locations, all of which are uncertain at the moment 2. Neutrinos!! No electric charge. Coming to us straight Highly complementary ν can travel over a LONG distance The cons : measurement of ν s is really a tough business They are weakly interacting particles a huge detector The atmospheric ν or μ backgrounds dominates needs excellent filtering programs Main topic in this talk
8 black hole radiation enveloping black hole
9
10 The highest energy neutrinos cosmogenic (GZK) neutrinos induced by the interactions of cosmic-ray and CMBs Off-Source (<50Mpc) astrophysical neutrino production via GZK (Greisen-Zatsepin-Kuzmin) mechanism p >100EeV π + ν μ ν μ ν e π 0 μ + e + Takami et al Astropart.Phys. 31, 201 (2009) The main energy range: E ν ~ GeV pγ K π + X μ + ν e + ' s 2.7 ν The region of the main GZK ν intensity Trace the UHECR emission history Probe maximal radiated energy Probe transition from galactic to extra-galactic Ahlers et al, Astropart.Phys (2010) Dip model Ankle model
11 Tracing history of the particle emissions with ν flux Intensity gets higher if the emission is more active in the past because ν beams are penetrating over cosmological distances ν rare frequent color : emission rate of ultra-high energy particles Present Redshift (z) Past The cosmological evolution Many indications that the past was more active. Hopkins and Beacom, Astrophys. J (2006) The spectral emission rate ρ(z) ~ (1+z) m Star formation rate m= 0 : No evolution
12 Tracing history of the particle emissions with ν flux ρ ~ (1+z) m 0<z<z max Decerprit and Allard, A&A (2012) Yoshida and Ishihara, PRD 85, (2012)
13 The ν spectra from cosmos and atmosphere SN relic ν solar ν atmospheric on-source ν ex. AGN, GRB off-source ν GZK cosmogenic
14 The IceCube Neutrino Observatory Completed: Dec : Project Start 1 string 2011: Project completion 86 strings Configuration chronology 2006: IC9 2007: IC : IC : IC : IC : IC86 PMT Full operation with all strings since May 2011 Digital Optical Module (DOM)
15
16 Topological signatures of IceCube events Down-going track atmospheric μ secondary produced μ from ν μ τ from ν >> PeV Up-going track atmospheric ν μ Cascade (Shower) directly induced by ν inside the detector volume via CC from ν e via NC from ν e, ν μ,ν τ all 3 flavor sensitive
17 IC strings May/31/2010-May/12/2011 Effective livetime days The dataset IC86 published PRD (2011) strings May/13/2011-May14/2012 Effective livetime days 9 strings (2006) 22 strings (2007) 40 strings (2008) 59 strings (2009) 79 strings (2010) 86 strings (2011)
18 Data Filtering at South Pole PY 2012 season 86 strings ~ the completed IceCube 2 nd level trigger Simple Majority Trigger 8 folds with 5 μ sec ~ 2.8 khz Muon Filter selects up-going tracks ~40 Hz EHE Filter selects bright events ~1 Hz NPE > 1000 p.e. Cascade Filter selects cascade -like events ~34 Hz Many others Min Bias Moon IceTop etc To Northern Hemisphere
19 Ultra-high Energy ν search Energy IceCube Depth Detection Principle Zenith IceCube Depth through-going track Secondary μ and τ from ν Sensitive to starting track/ cascade ν μ ν τ Directly induced events from ν Sensitive to ν e ν μ ν τ Yoshida et al PRD (2004) And tracks arrive horizontally
20 Ultra-high Energy ν search Detection Principle up-going down-going Energy Signal Domain atmospheric μ (bundle) atmospheric ν The blind analysis scheme cos(zenith) Use 10% of the data (test-sample) with masking the rest of them in optimizing the search algorithm with MC simulation
21 IC79 On the Analysis level The final-level selection criteria in the plain of NPE-cos(zenith) Number of events (z-axis) per the test-sample livetime test-sample data atmospheric μ atmospheric ν signal GZK ν conventional only IC86
22 Before reaching to this level Introduced multi-staged filtering/quality cuts ensured the simulations reasonably describe the test-sample data at each of the filter levels EHE filter level NPE>1000 Analysis level hit cleanings recalculation of NPEs NPE>3,200 NDOM>300 zenith angle reconstruction Final level > NPE threshold (cos(zenith)) # of events IC79(285.8days) + IC86 (330.1 days) Experimental data Background MC Signal MC atmospheric μ bundle atmospheric ν GZK ν Yoshida & Teshima (1993) 1.00 x x x x Note: assuming the pure Fe UHECR yielding the higher rate See the following slides +56.7% % conventional only +13.6% % NPE cos(zenith) % +68.7% plus the atmospheric prompt ν
23 Background Breakdown Total background (IC79+IC86) atmospheric muon atmospheric conventional neutrino atmospheric prompt neutrino Atmospheric μ Atmospheric ν (Conventional) Coincidence μ Total prompt ν Total with prompt (0.0823) excluding the testsample livetime
24 The systematic uncertainties on the BG rate +43.1% Detector efficiency -26.1% remarks absolute PMT/DOM calibration Ice properties/detector response -41.7% in-situ calibration by laser Cosmic-ray flux variation Cosmic-ray composition Hadronic interaction model ν yield from cosmic-ray nucleon +18.7% -26.3% -36.7% +8.1% +2.2% -2.2% UHECRs : HiRes Auger Uncertainties on The Knee spectrum The baseline to calculate atm μ: 100% Fe Compared against the pure proton case The baseline : Sibyll 2.1 Compared to QGSJET II - 03 The Elbert model prompt ν model +12.6% -16.1% The Enberg model perturbative-qcd
25 Effective Areas Area x ν flux x 4π x livetime = event rate IC79+IC86 livetime days ν ν e larger below 10 PeV due to effective energy deposition by showers μ τ dominant above 100 PeV due to the secondary produced μ and τ tracks τ s are no longer short-lived particles in EeV
26 Two events passed the final criteria 2 events / days (excluding the test-sample livetime) The Expected Backgrounds p-value 2.9x10-3 (2.8σ) including prompt conventional only p-value 9.0x10-4 (3.1σ) Run Event August 9 th 2011 ( Bert ) NPE x10 4 Number of Optical Sensors 354 Super-nicely contained cascades! Run Event Jan 3 rd 2012 ( Ernie ) NPE 9.628x10 4 Number of Optical Sensors 312
27 Recorded pulses Clean and luminous bulk of photons!! The Jan 2012 event - Ernie The Aug 2011 event - Bert 27
28 What are their energies? Maximizing the Poisson likelihood based on the recorded waveforms Estimated Energy Deposit Jan 2012 event (Ernie) 1.04 PeV Aug 2011 event (Bert) 1.14 PeV +- 15% accuracy zenith 11deg zenith 70deg A PeV shower
29 The GZK cosmogenic ν? The low Energy enhanced GZK scenarios Stronger IR/UV yield at high redshift Assume dip type transition of UHECRs from galactic to extragalactic Ex. Kotera et al JCAP (2010) p + IR/UV ν p + CMB ν The Standard GZK scenarios The CMB collisions dominates in streaming ν EeV (=10 9 GeV) is the key energy region
30 The KS Test Theme #1 p = The energies of Bert & Ernie is consistent with the expectations from the GZK scenario? Use the Kolmogorov-Smirnov statistics Take the energy uncertainty of Bert&Ernie into account dloge Bert ρ Bert(logEBert) dlogeernie ρ Erine(logE Ernie ) P KS (loge Bert,logE Ernie ) Energy PDF of Bert Energy PDF of Ernie KS statistical significance assuming the GZK ν spectrum to derive the PDF The standard GZK The low energy GZK p-value 7.5x10-2 p-value 3.9x10-2 inconsistent at >90% C.L. (not 99% CL)
31 Summarized statements on the origin of the 2 events if astrophysical (very likely, but not conclusive) They are unlikely to be GZK cosmogenic ν emission from cosmic-ray sources responsible for these two events are NOT extending above 100 PeV we would have detected events with greater energies, otherwise ν e+μ+τ intensity of ~ 10-8 GeV/cm2 sec sr Needs more data/follow-up analyses for further interpretation
32 The executive summary The model-independent upper limit on flux in UHE null observation in this regime nearly exclude radio-loud AGN jets m>4 for (1+z) m emission maximally allowed by the Fermi γ all flavor sum Bert & Ernie 2.8 σ excess over atmospheric
33 A search for events originated within the detector interior look for only events with their interaction vertices within the fiducial volume Bert & Ernie
34 Effective Areas expanding down to 100 TeV s Area x ν flux x 4π x livetime = event rate IC79+IC86 livetime days
35 sub-pev ν samples Bert & Ernie Bert & Ernie
36 sub-pev ν samples 28 events observed against bg of (4.1σ excess) Bert & Ernie φ νe+μ+τ (E)~(3.6 E ) x 10-8 [GeV/cm 2 sec sr]
37 sub-pev ν samples Bert Bert & Ernie Gal.Center The hottest spot (p-value 8% - NOT statistically significant)
38 The executive summary The model-independent upper limit on flux in UHE null observation in this regime nearly exclude radio-loud AGN jets m>4 for (1+z) m emission maximally allowed by the Fermi γ all flavor sum Bert & Ernie + O(10) sub-pev events 4.1 σ excess over atmospheric
39 Tracing history of the particle emissions with ν flux Intensity gets higher if the emission is more active in the past because ν beams are penetrating over cosmological distances ν rare frequent color : emission rate of ultra-high energy particles Present Redshift (z) Past The cosmological evolution Many indications that the past was more active. Hopkins and Beacom, Astrophys. J (2006) The spectral emission rate ρ(z) ~ (1+z) m Star formation rate m= 0 : No evolution
40 Constraints on UHECR origin The model-independent upper limit on flux ν e+μ+τ any model adjacent to the limit is disfavored by the observation Effective ν e+μ+τ detection exposure 6x10 7 m 2 days 1EeV = 0.2 km 2 sr year ( 6 x Auger ν τ exposure) Note: φ CR (>1EeV) ~ 20/km 2 sr year ν with CR comparable flux should have been detected
41 ν Model Rate >100PeV Model Rejection Factor Constraints on UHECR origin model-dependent limit based on the rate >100 PeV comparison to the nearly ~0 events in the present data GZK Y&T m=4,zmax=4 GZK Sigl m=5, zmax=3 GZK Ahler Fermi Best GZK Ahler Fermi Max GZK Kotera FR-II GZK Kotera SFR/GRB Topdown GUT p-value 1.4x x x x x x x10-2 Excluded Mildly Excluded Consistent Maximal ν flux allowed by the Fermi γ-ray measurement Ruled out relatively strong evolved sources if UHECRs are proton-dominated
42 Ultra-high energy ν intensity depends on the emission rate in far-universe Yoshida and Ishihara, PRD 85, (2012) intensity above 1 EeV(=10 18 ev) more than an order of magnitude difference quiet dynamic particle emissions in far-universe
43 GZK-CMB ν 1EeV Measurements of the evolution Yoshida and Ishihara, PRD 85, (2012) ρ ~ (1+z) m 0<z<z max GZK(-CMB) ν flux x IceCube Exposure Number of events we should have detected Evolution of UHECR sources Identify classes of astronomical objects responsible for UHECRs
44 Constraints on the evolution emission rate per co-moving volume ρ ~ (1+z) m 0<z<z max 90% C.L. = 3.3 evens above 100PeV 68% C.L. = 1.9 evens above 100PeV A strongly evolved astronomical object (like FR-II radio galaxy) has already been disfavored any scenario involving sources evolved stronger than SFR will soon be ruled out by IceCube if we see no events in EeV rage. gives the best fit with UHECR spectrum radio laud AGN star formation rate GRB Note: Not precisely known 46
45 Ultra-high energy ν intensity depends on the emission rate in far-universe intensity more than an order of magnitude difference
46 WIMP from Sun Bert & Ernie
47 WIMP from Sun Bert & Ernie
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